Instability and new phases of higher-dimensional rotating black holes

By Ó. J. Dias, Pau Figueras, R. Monteiro, Jorge E Santos, Roberto Emparan. 2009

146 citations recorded by the source corpus.

It has been conjectured that higher-dimensional rotating black holes become unstable at a sufficiently large value of the rotation, and that new black holes with pinched horizons appear at the threshold of the instability. We search numerically and find the stationary axisymmetric perturbations of Myers-Perry black holes with a single spin that mark the onset of the instability and the appearance of the new black hole phases. We also find new ultraspinning Gregory-Laflamme instabilities of rotating black strings and branes.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/b79b14a9ed47dc04e51816e5ae636edeba8a7760

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Citations in the corpus

Superradiance: Energy Extraction, Black-Hole Bombs and Implications for Astrophysics and Particle Physics (2015, background): “As another example, for D ≥ 6 dimensions where no upper bound on the rotation of Myers-Perry BHs exists, a Gregory-Laflammelike instability renders ultra-spinning BHs unstable [378, 379, 380, 381, 382].”
Numerical methods for finding stationary gravitational solutions (2015, methodology): “At the time, the only known instability was the superradiant instability, but this proof applies much more broadly, such as to the Gregory-Laflamme instability of the (boosted) black string [113, 115, 116, 127–131, 135, 136, 420] and black ring [404], to the ultraspinning [128–131, 136, 397] and to ”
Superradiance (2015, background): “As another example, for D ≥ 6 dimensions where no upper bound on the rotation of Myers-Perry BHs exists, a Gregory-Laflamme-like instability renders ultra-spinning BHs unstable [548, 549, 550, 551, 552].”
Holographic thermalization, quasinormal modes and superradiance in Kerr-AdS (2013, background): “Indeed, it is established that D ≥ 6 stationary BHs are also unstable to the ultraspinning instability, whose onset was identified in [70] (this instability was first studied in asymptotically flat stationary BHs in D ≥ 6 [71, 72, 73, 67, 74]).”
Essentials of blackfold dynamics (2009, background): “It must be noted, though, that higher-dimensional neutral black holes exhibit zero-mode deformations at discrete values of the spin when n ≥ 3 (when n = 1, 2 such deformations appear to be always massive modes) [7].”
Thermodynamics of Rotating Black Holes and Black Rings: Phase Transitions and Thermodynamic Volume (2014, background): “However it has been conjectured [120] that the zero modes with k ≥ 2 can only occur for rotations higher than that of the k = 1 modes.”
Overdamped modes in Schwarzschild-de Sitter and a Mathematica package for the numerical computation of quasinormal modes (2017, methodology): “The method used was ﬁrst used for general relativity in [27–29].”
An instability of higher-dimensional rotating black holes (2010, methodology): “[4], where it is argued that the quantity of interest is the Hessian matrix Hij = (∂ (2)(−S)/∂Ji∂Jj)M where S is the black hole entropy.”